Shear viscosity of a highly excited string and black hole membrane - PowerPoint PPT Presentation

Shear viscosity of a highly excited string and black hole membrane paradigm Yuya Sasai Helsinki Institute of Physics and Department of Physics University of Helsinki in collaboration with A. Zahabi Based on arXiv:1010.5380 Accepted by PRD RIKEN symposium 2010 18 December 2010

1. Introduction Mysteries of black holes • Microscopic origin of Bekenstein-Hawking entropy (A: area of the event horizon) • Microscopic origin of membrane paradigm “A certain fictitious viscous membrane seems to be sitting on a stretched horizon for a distant observer .” Thorne, Price, Macdonald (1986) BH Stretched horizon We need a consistent quantum theory which includes gravity. String theory!

Bekenstein-Hawking entropy vs entropy of a fundamental string Entropy of a Logarithm of the number of fundamental string degeneracy of the string states For a highly excited free string, On the other hand, (d: Number of spatial dimensions) Clearly, in generic

Horowitz, Polchinski (1996) String-black hole correspondence Damour, Veneziano (1999) If , ! At this point, the horizon radius becomes If we increase adiabatically, a highly excited string becomes a black hole with at . =

Entropy of a macroscopic black hole from a fundamental string Susskind (1993) A large gravitational redshift of a black hole explains the difference between and . Consider a highly excited string on a stretched horizon of a Schwarzshild black hole. Due to the redshift, the energy for an observer at the stretched horizon is not the same as the energy for an asymptotic observer. BH

Derivation of Susskind (1993) (d+1)-dimensional Schwarzshild metric : Volume of a unit (d-1) sphere Near horizon geometry 2 dim. Rindler spacetime : Surface gravity

To find the energy and temperature for an observer at , it is convenient to introduce dimensionless Rindler quantities. Define the Rindler time Rindler energy is conjugate to is conjugate to Thus, By using the first law of thermodynamics, we obtain the Rindler temperature

The proper time at is The stretched horizon is defined by the place where the local Unruh temperature is given by the Hagedorn temperature The stretched horizon is located at .

Consistency with the string-black hole correspondence If the redshift factor is of the order of one, This is the same situation as the string-black hole correspondence. In this case, the energy and temperature for an observer on the stretched horizon are of the same order as those for the asymptotic observer.

Membrane paradigm from the viewpoint of a fundamental string Can we reproduce the viscosity of the fictitious membrane from a highly excited BH string? What is the viscosity of the string? In polymer physics, This is due to the fact that the stress tensor of the polymer itself is added to the stress tensor of the solvent.

Contents 1. Introduction 2. Open string in highly excited states 3. Shear viscosity of a highly excited string 4. Shear viscosity of a string on a stretched horizon and black hole membrane paradigm 5. Summary and comments

2. Open string in highly excited states Review of bosonic open string Worldsheet action in flat background spacetime Choosing the unit gauge, , the action becomes where .

Mode expansion of for open string where . We choose the light-cone gauge, Mass shell condition where ( )

Observables in highly excited string states Damour, Veneziano (1999) In terms of the usual harmonic oscillators, The level of the open string becomes Number operator Consider the following “canonical partition function” ,

Since the density matrix is defined by , an expectation value of an observable is evaluated by ( : Observable) The mean value of the level and the fluctuation If , we can obtain observables in highly excited string states.

Mass of the string Entropy of the string This is consistent with the Cardy formula, (c : central charge) with

3. Shear viscosity of a highly excited string Stress tensor of the open string Source term After Insertion of the light-cone gauge and integration over , with

Since the stress tensor trivially vanishes outside the string sizes, we restrict the ranges of the spatial coordinates as follows: where we have chosen . For free open string,

To obtain the viscosity, we just have to consider the long wave length limit. Zero modes for spatial directions Fourier expansions of the delta functions Zero mode of the stress tensor where

Kubo’s formula for shear viscosity (We have assumed that nonvanishing components of the metric perturbation are and they only depend on .) Using , We obtain

4. Shear viscosity of a string on a stretched horizon and black hole membrane paradigm Difference between fictitious membrane and highly excited string Membrane paradigm Highly excited string Distributed BH dimensional in spatial surface dimensions No radial thickness. Mass dimension of stress tensor Mass dimension of shear viscosity We consider the longitudinally reduced stress tensor of the string.

Longitudinally reduced stress tensor The stress tensor of the string can be written as . We define the longitudinally reduced stress tensor (Mass dimension = d) The zero mode of for the transverse directions

Shear viscosity of the longitudinally reduced string Since the shear viscosity of the longitudinally reduced string is where is the volume of the transverse size of the string. does not change if the string is longitudinally reduced because this quantity is dimensionless.

Shear viscosity of the longitudinally reduced string on the stretched horizon Shear viscosity of the longitudinally reduced string in the flat background BH On the stretched horizon, we have to replace , This is consistent with the membrane paradigm

Consistency with string-black hole correspondence If , a highly excited string becomes a black hole with . At the critical string coupling, the shear viscosity of the string will be On the other hand, the shear viscosity in the membrane paradigm becomes Consistent!

About the ratio of the shear viscosity to entropy density In our estimate, does not change even if we put the string on the stretched horizon. On the other hand, If , of the string matches with that of the membrane paradigm.

5. Summary and comments • We have obtained the shear viscosity and of the highly excited string by using the Kubo’s formula. • We have estimated the shear viscosity and of the string on the stretched horizon of the black hole. • The results are consistent with the black hole membrane paradigm.

• We have not considered the self-interactions of the highly excited string. This will lead to the corrections to shear viscosity. • It is important to investigate whether the correct numerical coefficient of the shear viscosity in the membrane paradigm can be derived from superstring theory. • We have not discussed the bulk viscosity because we could not reproduce the negative bulk viscosity of the membrane paradigm from the highly excited string on the stretched horizon. • It is interesting to find transport coefficients of a highly excited string when source fields are given by other fields instead of metric.